Convolves the current spectrum with the line shape from the kerrdisk model. A detailed description can be found in Brenneman & Reynolds (2006). This model is quite slow so is best used after models such as laor or diskline have been employed to get an estimate of the best-fit parameters.
|par1||emissivity index for the inner disk|
|par2||emissivity index for the outer disk|
|par3||break radius separating the inner and outer portions of the disk (gravitational radii)|
|par4||dimensionless black hole spin|
|par5||disk inclination angle to the line of sight (degrees)|
|par6||inner radius of the disk in units of the radius of marginal stability|
|par7||outer radius of the disk in units of the radius of marginal stability|